학술논문
UV-Bright Star-Forming Clumps and Their Host Galaxies in UVCANDELS at 0.5 $\leq$ z $\leq$ 1
Document Type
Working Paper
Author
Martin, Alec; Guo, Yicheng; Wang, Xin; Koekemoer, Anton M.; Rafelski, Marc; Teplitz, Harry I.; Windhorst, Rogier A.; Alavi, Anahita; Grogin, Norman A.; Prichard, Laura; Sunnquist, Ben; Ceverino, Daniel; Chartab, Nima; Conselice, Christopher J.; Dai, Y. Sophia; Dekel, Avishai; Gardner, Johnathan P.; Gawiser, Eric; Hathi, Nimish P.; Hayes, Matthew J.; Jansen, Rolf A.; Ji, Zhiyuan; Koo, David C.; Lucas, Ray A.; Mandelker, Nir; Mehta, Vihang; Mobasher, Bahram; Nedkova, Kalina V.; Primack, Joel; Ravindranath, Swara; Robertson, Brant E.; Rutkowski, Michael J.; Sattari, Zahra; Soto, Emmaris; Yung, L. Y. Aaron
Source
ApJ 955 106 (2023)
Subject
Language
Abstract
Giant star-forming clumps are a prominent feature of star-forming galaxies (SFGs) and contain important clues on galaxy formation and evolution. However, basic demographics of clumps and their host galaxies remain uncertain. Using the HST/WFC3 F275W images from the Ultraviolet Imaging of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (UVCANDELS), we detect and analyze giant star-forming clumps in galaxies at 0.5 $\leq$ z $\leq$ 1, connecting two epochs when clumps are common (at cosmic high-noon, z $\sim$ 2) and rare (in the local universe). We construct a clump sample whose rest-frame 1600 {\AA} luminosity is 3 times higher than the most luminous local HII regions (M$_{UV} \leq -$16 AB). In our sample, 35 $\pm$ 3$\%$ of low-mass galaxies (log[M$_{*}$/M$_{\odot}$] $<$ 10) are clumpy (i.e., containing at least one off-center clump). This fraction changes to 22 $\pm$ 3$\%$ and 22 $\pm$ 4$\%$ for intermediate (10 $\leq$ log[M$_{*}$/M$_{\odot}$] $\leq$ 10.5) and high-mass (log[M$_{*}$/M$_{\odot}$] $>$ 10.5) galaxies in agreement with previous studies. When compared to similar-mass non-clumpy SFGs, low- and intermediate-mass clumpy SFGs tend to have higher SFRs and bluer rest-frame U-V colors, while high-mass clumpy SFGs tend to be larger than non-clumpy SFGs. However, clumpy and non-clumpy SFGs have similar S\'ersic index, indicating a similar underlying density profile. Furthermore, we investigate how UV luminosity of star-forming regions correlates with the physical properties of host galaxies. On average, more luminous star-forming regions reside in more luminous, smaller, and/or higher-specific SFR galaxies and are found closer to their hosts' galactic center.
Comment: 21 pages, 13 figures, accepted for publication in ApJ
Comment: 21 pages, 13 figures, accepted for publication in ApJ